Aoki, W.; Honda, S.; Beers, T. C.; Takada-Hidai, M.; Iwamoto, N.; Tominaga, N.; Umeda, H.; Nomoto, K.; Norris, J. E. and Ryan, S. G.
|DOI (Digital Object Identifier) Link:||https://doi.org/10.1086/512601|
|Google Scholar:||Look up in Google Scholar|
detailed elemental abundance analysis has been carried out for the very metal-poor (Fe/H = -2.7)star BS 16934-002, which was identified in our previous work as a star exhibiting large overabundances of Mg and Sc. A comparison of the abundance pattern of this star with that of the well-studied metal-poor star HD 122563 indicates excesses of O, Na, Mg, Al, and Sc in BS 16934 002. Of particular interest, no excess of C or N is found in this object, in contrast to CS 22949-037 and CS 29498-043, two previously known carbon-rich, extremely metal-poor stars with excesses of the alpha-elements. No established nucleosynthesis model exists that explains the observed abundance pattern of BS 16934-002. A supernova model, including mixing and fallback and assuming severe mass loss before explosion, is discussed as a candidate progenitor of BS 16934-002.
|Item Type:||Journal Article|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Depositing User:||Colin Smith|
|Date Deposited:||24 Apr 2009 09:04|
|Last Modified:||04 Oct 2016 10:20|
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